<i>Chandra</i>ACIS Spectroscopy of N157B: A Young Composite Supernova Remnant in a Superbubble

Chen, Yang; Wang, Q. Daniel; Gotthelf, E. V.; Jiang, Bin; Chu, You‐Hua; Gruendl, R. A.

doi:10.1086/507017

Cited by 78 publications

(76 citation statements)

References 59 publications

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“…Given a lack of plerionic remnants in the SMC we can use the LMC for comparison. PWN containing remnants in the LMC typically have a lower index: α = 1.0 ± 0.2 in SNR 0453-68. for DEM L241 (Bamba et al 2006); and α ∼ 1.2 − 1.6 over several regions from N 157B (Chen et al 2006). At SMC distance the calculated luminosity would be consistent with that expected expected from a PWN.…”

Section: X-raysupporting

confidence: 80%

HFPK 334: An Unusual Supernova Remnant in the Small Magellanic Cloud

Crawford

Filipović

McEntaffer

et al. 2014

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We present new Australia Telescope Compact Array (ATCA) radio-continuum and XMM-Newton/Chandra X-ray Observatory (CXO) observations of the unusual supernova remnant HFPK 334 in the Small Magellanic Cloud (SMC). The remnant follows a shell type morphology in the radio-continuum and has a size of ∼20 pc at the SMC distance. The X-ray morphology is similar, however, we detect a prominent point source close to the center of the SNR exhibiting a spectrum with a best fit powerlaw with a photon index of Γ = 2.7 ± 0.5. This central point source is most likely a background object and cannot be directly associated with the remnant. The high temperature, nonequilibrium conditions in the diffuse region suggest that this gas has been recently shocked and point toward a younger SNR with an age of 1800 years. With an average radio spectral index of α = −0.59 ± 0.09 we find that an equipartition magnetic field for the remnant is ∼90 µG, a value typical of younger SNRs in lowdensity environments. Also, we report detection of scattered radio polarisation across the remnant at 20 cm, with a peak fractional polarisation level of 25±5%.

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Section: X-raysupporting

confidence: 80%

HFPK 334: An Unusual Supernova Remnant in the Small Magellanic Cloud

Crawford

Filipović

McEntaffer

et al. 2014

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“…On the other hand, much more pronounced spectral softening trends have been measured in the N157B (∆Γ ≈ 1.3, Chen et al 2006), the Lighthouse (∆Γ ≈ 0.7, Pavan et al 2016), and the Mouse (Gaensler et al 2004; ∆Γ ≈ 1.5, Klingler et al in prep) PWNe.…”

Section: Stem and Tailmentioning

confidence: 95%

“…One can also use a simple 1D model of a collimated outflow cooling solely via synchrotron radiation (e.g., Chen et al 2006) to estimate the flow speed. In a cylindrical tail where particles flow away from the pulsar with a constant velocity u in a constant magnetic field B, the photon index at distance z from the pulsar can be ex-pressed as…”

Section: Physical Propertiesmentioning

confidence: 99%

Deep Chandra Observations of the Pulsar Wind Nebula Created by PSR B0355+54

Klingler

Rangelov

Kargaltsev

et al. 2016

ApJ

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We report on Chandra X-ray Observatory (CXO) observations of the pulsar wind nebula (PWN) associated with PSR B0355+54 (eight observations with a 395 ks total exposure, performed over an 8 month period). We investigated the spatial and spectral properties of the emission coincident with the pulsar, compact nebula (CN), and extended tail. We find that the CN morphology can be interpreted in a way that suggests a small angle between the pulsar spin axis and our line-of-sight, as inferred from the radio data. On larger scales, emission from the 7 (≈ 2 pc) tail is clearly seen. We also found hints of two faint extensions nearly orthogonal to the direction of the pulsar's proper motion. The spectrum extracted at the pulsar position can be described with an absorbed power-law + blackbody model. The nonthermal component can be attributed to magnetospheric emission, while the thermal component can be attributed to emission from either a hot spot (e.g., a polar cap) or the entire neutron star surface. Surprisingly, the spectrum of the tail shows only a slight hint of cooling with increasing distance from the pulsar. This implies either a low magnetic field with fast flow speed, or particle re-acceleration within the tail. We estimate physical properties of the PWN and compare the morphologies of the CN and the extended tail with those of other bow shock PWNe observed with long CXO exposures.

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“…PSR J0537−6910 is a 16 ms pulsar associated with the ∼5000-year old SNR 0537.8−6910 and PWN N 157B 7 . The whole system presumably results from the explosion of a ∼25 M O8-O9 star and is likely associated with the OB association LH99 (Chen et al 2006;Micelotta et al 2009). The pulsar was discovered from X-ray observations (Marshall et al 1998) and is the most rapidly spinning and the most powerful young pulsar known, with a spin-down luminosity ofĖ = 4.9 × 10 38 erg s −1 .…”

Section: P2: Coincident With Psr J0537−6910/n 157bmentioning

confidence: 99%

Deep view of the Large Magellanic Cloud with six years ofFermi-LAT observations

Ackermann¹,

Albert²,

Atwood³

et al. 2016

A&A

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Context. The nearby Large Magellanic Cloud (LMC) provides a rare opportunity of a spatially resolved view of an external star-forming galaxy in γ-rays. The LMC was detected at 0.1-100 GeV as an extended source with CGRO/EGRET and using early observations with the Fermi-LAT. The emission was found to correlate with massive star-forming regions and to be particularly bright towards 30 Doradus. Aims. Studies of the origin and transport of cosmic rays (CRs) in the Milky Way are frequently hampered by line-of-sight confusion and poor distance determination. The LMC offers a complementary way to address these questions by revealing whether and how the γ-ray emission is connected to specific objects, populations of objects, and structures in the galaxy. Methods. We revisited the γ-ray emission from the LMC using about 73 months of Fermi-LAT P7REP data in the 0.2-100 GeV range. We developed a complete spatial and spectral model of the LMC emission, for which we tested several approaches: a simple geometrical description, template-fitting, and a physically driven model for CR-induced interstellar emission. Results. In addition to identifying PSR J0540−6919 through its pulsations, we find two hard sources positionally coincident with plerion N 157B and supernova remnant N 132D, which were also detected at TeV energies with H.E.S.S. We detect an additional soft source that is currently unidentified. Extended emission dominates the total flux from the LMC. It consists of an extended component of about the size of the galaxy and additional emission from three to four regions with degree-scale sizes. If it is interpreted as CRs interacting with interstellar gas, the large-scale emission implies a large-scale population of ∼1-100 GeV CRs with a density of ∼30% of the local Galactic value. On top of that, the three to four small-scale emission regions would correspond to enhancements of the CR density by factors 2 to 6 or higher, possibly more energetic and younger populations of CRs compared to the large-scale population. An alternative explanation is that this is emission from an unresolved population of at least two dozen objects, such as pulsars and their nebulae or supernova remnants. This small-scale extended emission has a spatial distribution that does not clearly correlate with known components of the LMC, except for a possible relation to cavities and supergiant shells. Conclusions. The Fermi-LAT GeV observations allowed us to detect individual sources in the LMC. Three of the newly discovered sources are associated with rare and extreme objects. The 30 Doradus region is prominent in GeV γ-rays because PSR J0540−6919 and N 157B are strong emitters. The extended emission from the galaxy has an unexpected spatial distribution, and observations at higher energies and in radio may help to clarify its origin.

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ChandraACIS Spectroscopy of N157B: A Young Composite Supernova Remnant in a Superbubble

Cited by 78 publications

References 59 publications

HFPK 334: An Unusual Supernova Remnant in the Small Magellanic Cloud

HFPK 334: An Unusual Supernova Remnant in the Small Magellanic Cloud

Deep Chandra Observations of the Pulsar Wind Nebula Created by PSR B0355+54

Deep view of the Large Magellanic Cloud with six years ofFermi-LAT observations

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